As discussed in [1]}, the line widths (at 10 and 50 % of the maximum) of the profiles in Figures REF  and REF 
reflect both the temperature of the region at which most of the line is formed
as well as the absorption by the layers above this in the postshock region. We can now extend this statement by noting that the accretion flow too can change the width of the line, for \(\dot{M} >3\times 10^{-5}\)  (\(3\times 10^{-3}\) ) \(M_{\mathrm {J}}\,\mathrm {yr}^{-1}\)  in the SpherAcc (Polar) case.
